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arXiv 1901.07971astro-ph.SRphysics.space-ph
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日冕中快速强迫重联的观测

On the observations of rapid forced reconnection in the solar corona

A. K. Srivastava, Sudheer K. Mishra, P. Jelínek, Tanmoy Samanta, Hui Tian, Vaibhav Pant, P. Kayshap, D. Banerjee, J. G. Doyle, B. N. Dwivedi

备注：
14 Pages; 07 Figures; The Astrophysical Journal (in press)
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摘要：

利用2012年5月3日太阳动力学天文台（SDO）上的大气成像组件（AIA）的多波长成像观测，我们提出了一个新的物理场景，在日冕中形成一个临时的X点，在那里等离子体动力学是由移动的日珥迫使外部。自然扩散并不占主导地位，然而，突出驱动的流入首先发生，形成薄电流片，然后使强制磁重联在一个相当高的速度。数值模型的观测结果表明，强迫重联可能会迅速和有效地发生在更高的速率在太阳日冕。这种物理过程也可以局部加热日冕，即使没有建立一个重要的和自洽的扩散区域。使用参数的数值研究，我们表明，外部驱动器的实现增加了重连的速率，即使当创建正常扩散区所需的电阻率在X点降低。我们推测，适当的外力可以使相反方向的场线进入临时创建的扩散区，首先通过等离子体流入的观察。此后，重连和相关的等离子体流出可能以相当大的速率发生。

英文摘要：

Using multiwavelength imaging observations from the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) on 03 May 2012, we present a novel physical scenario for the formation of a temporary X-point in the solar corona, where plasma dynamics is forced externally by a moving prominence. Natural diffusion was not predominant, however, a prominence driven inflow occurred firstly, forming a thin current sheet and thereafter enabling a forced magnetic reconnection at a considerably high rate. Observations in relation to the numerical model reveal that forced reconnection may rapidly and efficiently occur at higher rates in the solar corona. This physical process may also heat the corona locally even without establishing a significant and self-consistent diffusion region. Using a parametric numerical study, we demonstrate that the implementation of the external driver increases the rate of the reconnection even when the resistivity required for creating normal diffusion region decreases at the X-point. We conjecture that the appropriate external forcing can bring the oppositely directed field lines into the temporarily created diffusion region firstly via the plasma inflows as seen in the observations. The reconnection and related plasma outflows may occur thereafter at considerably larger rates.

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